Cosmological models based on a complex scalar field with a power-law potential associated with a polytropic equation of state

Abstract

We construct cosmological models based on a complex scalar field with a power-law potential $V=\frac{K}{\gamma -1}(\frac{m}{\hslash }{)}^{2\gamma }|\phi {|}^{2\gamma }$ associated with a polytropic equation of state $P=K{\rho }^{\gamma }$ (the potential associated with an isothermal equation of state $P=\rho k_{B}T/m$ is $V=\frac{m{k}_{B}T}{{\hslash }^2}|\phi {|}^2[\ln (m^2|\phi {|}^2/{\rho }_{\ast }{\hslash }^2)-1]$ and the potential associated with a logotropic equation of state $P=A\ln (\rho /{\rho }_P)$ is $V=-A[\ln (m^2|\phi {|}^2/{\hslash }^2{\rho }_P)+1]$). We consider a fast oscillation regime of ``spintessence'' where the equations of the problem can be simplified. We study all possible cases with arbitrary (positive and negative) values of the polytropic constant and polytropic index. The $\Lambda$CDM model, the Chaplygin gas model and the Bose-Einstein condensate model are recovered as particular cases of our study corresponding to a constant potential ($\gamma =0$), an inverse square-law potential ($\gamma =-1$), and a quartic potential ($\gamma =2$). We also derive the two-fluid representation of the Chaplygin gas model.

References in corpus (64)

• Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
• Measurements of Omega and Lambda from 42 High-Redshift Supernovae
• Cosmological Imprint of an Energy Component with General Equation of State
• A Phantom Menace? Cosmological consequences of a dark energy component with super-negative equation of state
• Where are the missing galactic satellites?
• An alternative to quintessence
• A Flat Universe from High-Resolution Maps of the Cosmic Microwave Background Radiation
• Phantom Energy and Cosmic Doomsday
• A Dynamical Solution to the Problem of a Small Cosmological Constant and Late-time Cosmic Acceleration
• k-Inflation
• Cold and Fuzzy Dark Matter
• Ultralight scalars as cosmological dark matter
• Kinetically Driven Quintessence
• Too big to fail? The puzzling darkness of massive Milky Way subhaloes
• MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on angular scales of 10 arcminutes to 5 degrees
• Cold collapse and the core catastrophe
• Perturbations in k-inflation
• Accelerated expansion of the universe driven by tachyonic matter
• Unification of Dark Matter and Dark Energy: the Inhomogeneous Chaplygin Gas
• Cosmology with Ultra-light Pseudo-Nambu-Goldstone Bosons
• Cosmological Evolution of a Quintom Model of Dark Energy
• Field Theory of Tachyon Matter
• Cosmological Evolution of the Rolling Tachyon
• Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions: I. Analytical results
• Can the clustered dark matter and the smooth dark energy arise from the same scalar field ?
• Ultra-Light Dark Matter
• The end of unified dark matter?
• Tachyons, Scalar Fields and Cosmology
• Power-Law Inflation from the Rolling Tachyon
• A Further Analysis of a Cosmological Model of Quintessence and Scalar Dark Matter
• Prospects and Problems of Tachyon Matter Cosmology
• Bose-Einstein Condensate general relativistic stars
• The dearth of halo dwarf galaxies: is there power on short scales?
• Electroweak Baryogenesis and the Expansion Rate of the Universe
• Cosmology with a stiff matter era
• Cosmological Constraints on Bose-Einstein-Condensed Scalar Field Dark Matter
• Spintessence! New Models for Dark Matter and Dark Energy
• Growth of perturbations in an expanding universe with Bose-Einstein condensate dark matter
• Phase transitions between dilute and dense axion stars
• Noninteracting dark matter
• Dynamical and Gravitational Instability of Oscillating-Field Dark Energy and Dark Matter
• Shape invariance method for quintom model in the bent brane background
• Can the quintessence be a complex scalar field?
• Cosmological constraints on quintessential halos
• The Logotropic Dark Fluid as a unification of dark matter and dark energy
• Hydrodynamic representation of the Klein-Gordon-Einstein equations in the weak field limit: I. General formalism and perturbations analysis
• Cosmological evolution of a complex scalar field with repulsive or attractive self-interaction
• Models of dark matter halos based on statistical mechanics: II. The fermionic King model
• A predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere
• Models of dark matter halos based on statistical mechanics: I. The classical King model
• Cosmological perturbations in coherent oscillating scalar field models
• Relativistic self-gravitating Bose-Einstein condensates and cold baryons with a stiff equation of state
• The $\Lambda \mathrm{CDM}$ Limit of the Generalized Chaplygin Gas Scenario
• Difficulty of a spinning complex scalar field to be dark energy
• Constraints on anharmonic corrections of Fuzzy Dark Matter
• Jeans type instability of a complex self-interacting scalar field in general relativity
• Jeans mass-radius relation of self-gravitating Bose-Einstein condensates and typical parameters of the dark matter particle
• ASYMPTOTIC BEHAVIOR OF COMPLEX SCALAR FIELDS IN A FRIEDMAN-LEMAITRE UNIVERSE
• A heuristic wave equation parameterizing BEC dark matter halos with a quantum core and an isothermal atmosphere
• Time evolution of the perturbations for a complex scalar field in Friedmann-Lemaitre universe
• Quantum tunneling rate of dilute axion stars close to the maximum mass
• Non-Relativistic Formation of Scalar Clumps as a Candidate for Dark Matter
• Observational constraints on complex quintessence with attractive self-interaction
• K-essence Lagrangians of polytropic and logotropic unified dark matter and dark energy models

Cited by in corpus (3)

• Maximum mass of relativistic self-gravitating Bose-Einstein condensates with repulsive or attractive $|\phi {|}^4$ self-interaction
• A new logotropic model based on a complex scalar field with a logarithmic potential
• Complex Inflaton Potentials with Nonminimal Coupling: Robust Inflation and Geometric Reheating